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HEATING OF THE PARTIALLY IONIZED SOLAR CHROMOSPHERE BY WAVES IN MAGNETIC STRUCTURES

  • Authors: S. Shelyag, E. Khomenko, A. de Vicente, and D. Przybylski

2016 The Astrophysical Journal Letters 819 L11.

  • Provider: AAS Journals

Caption: Figure 4.

Conversion into thermal energy of the static currents and the currents induced by oscillatory perturbation in the domain. Left panel: evolution of the kinetic (blue), magnetic (red) and thermal (black) energies averaged over the volume of the numerical domain bounded by the surface ﹩\beta \lt 1﹩ within the flux tube for the AD simulation. The initial thermal and magnetic energy values have been subtracted. Right panel: evolution of the difference between the energies in the ADW simulation and AD and W simulations. Dashed curve corresponds to the absolute value of the sum of the magnetic and kinetic energy differences.

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